RHESSI Imaging on Short Timescales

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Revision as of 17:31, 13 December 2009

Introduction

Very little has been done to investigate RHESSI imaging capabilities on short time scales, even as long as the spacecraft rotation period of 4 s. I have begun to investigate this issue by looking at the decay of the 21 April 2002 event during the second orbit after 02:00 UT, when we can safely assume that the morphology of the flare is not changing significantly on such short time scales. Furthermore, the emission is primarily at energies below 20 keV and the source(s) are quite extended so there is little, if any, modulation by the finer grids.

Images in 4-second Time Intervals

Despite this belief that the source(s) will be extended, the pixon image for a random 4-s interval during this orbit shows several structures.

Pixon Image Analysis for 4-s Interval

Figure 1:'Pixon image for a 4-s time interval during the decay (2nd orbit) of the flare on 21 April 2002.‎

Figure 2:'Pixon modulation profiles for image shown in Fig. 1.

Note that despite the relatively small values of the C-statistic for all detectors, there are considerable differences between the measured count rates and the rates calculated from the image, especially for detector 9.

The pixon image for the next 4-s interval looks nothing like the first as shown in the next figure, where this second image is shown in color with the contours showing the first image.

Pixon Image Analysis for Next 4-s Interval

Figure 3:'Pixon image for the next 4-s time interval.

Figure 4:'Pixon modulation profiles for image shown in Fig. 3.

The pixon modulation profiles for this second 4-s interval look similar but note the several large data gaps for detector 8 and 9 and the significantly larger values of the C-statistic, with a value for detector 8 of 2.4. Also note that the predicted profile (the white curve) for detector 8 is shown during a data gap. Richard Schwartz has a fix for this problem by setting the control parameter, NO_CSA_DROPOUT to 1. This uses the absence of counts to identify gaps instead of a Charge Sensitive Amplifier (CSA) reset pulse, which indicates the dissipation of a large amount of charge in the germanium detector and the subsequent electronic saturation leading to a data gap. (Note that the time duration with zero counts to be called a data gap is controlled with the parameters named DP_CUTOFF... )

Source Location vs. Time Every 4 s

The location of the back-projection source determined for individual grids is shown as a function of time in the next figure. The top plot is for detector 8 and the bottom plot is for detector 9. Note that for most of the time intervals the scatter of the centroid location is of the order of 10 arcseconds but there are a couple of intervals in each case when the centroid is displaced by a much larger amount. It seems that this large displacement is the result of large or multiple data gaps for the individual detectors. Quite why this would result in such large offsets is being investigated.

The 1-sigma statistical error in the source location is given by the following equation taken from Hurford et al. (Apj. 595, L77, 2003):

Insertformulahere

σ = 2RN^0.5 / (πaS)

left|Figure 5:'X location of source peak vs. time for detector 8 (top) and detector 9 (bottom) taken from back projection images.

Images in 20-second Time Intervals

Pixon image for 20 s interval

Figure 6:'Pixon image for 20 s interval.

Figure 7:'Pixon modulation profiles for image shown in Fig. 6.